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Compara've Exoplanetology in the Era of the Great Observatories, JWST, and Beyond

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Compara've Exoplanetology in the Era of the Great Observatories, JWST, and Beyond Compara've Exoplanetology in the Era of the Great Observatories, JWST, and Beyond Jacob Bean University of Chicago University of Chicago Group – January 2017 University of Chicago Group – January 2017 Will start as a Fla>ron Research Fellow at the Simons Center for Computa>onal Astrophysics (NYC) in September Known exoplanets as of June 2017 N ≈ 5000 radial velocity transit direct imaging microlensing Fundamental Themes for Exoplanet Atmosphere Characteriza'on Determining thermal Measuring composi>ons to structures, energy budgets, trace planet forma>on and and dynamics to understand evolu>on. planetary physics. Connected ques>ons mo>vates holis>c studies. The “Small Black Shadow” vs. “The Pale Blue Dot” Strengths: • Know the mass and radius of the planet • Mul>ple probes of the atmosphere • Can study planets close-in to their host stars • Rapidly advancing field Weaknesses: • Measure planets rela>ve to their stars • Limited (for the most part) to planets that are transi>ng • Limited to close-in planets (a << 1 AU) Astronaut Andrew Feustel installs the Wide Field Camera 3 (May 14, 2009) Using an instrument designed for faint galaxies to look at bright, nearby stars spa>al direc>on spectral direc>on Probing Exoplanet Atmospheres With Transits We#observe#the)phase)varia3on#to#map# In# secondary# eclipse,# we# measure# the# dayside# emission) the# planet’s# emission) as) a) func3on) of) spectrum)of#the#planet#as#its#light#is#blocked#by#the#host# longitude.# This# probes# the# dynamics# of# star.# Emission# spectroscopy# is# sensi;ve# to# the# absolute# energy#transport.# chemical#abundances#and#the#thermal#structure.# In#transit,#we#measure#the#transmission)spectrum)of#the#planet#as# light# from# the# host# star# is# absorbed# by# chemical# species# in# the# planet’s# atmosphere.# These# data# are# most# sensi;ve# to# the# rela;ve# chemical#abundances#and#the#presence#of#cloud#or#haze#par;cles.# Robust modeling is cri>cal! phase 0.25 of WASP-43b Feng+ 2016 Key Ques>on #1: What are the metallici'es of planetary atmospheres? Key Ques>on #1: What are the metallici'es of planetary atmospheres? Fortney+ 2013, 100km planetesimals Precise Water Abundance for WASP-43b dayside'emission'spectrum' transmission) emission) combined) H2O) combined)result)gives)(1σ):) transmission'spectrum' O/H)=)0.4)–)3.5)x)solar!) (assuming)solar)abundance)rADos)) Kreidberg+ 2014b Key Ques>on #1: What are the metallici'es of planetary atmospheres? Exoplanet data: Kreidberg+ 2014b, Fraine+ 2014, Kreidberg+ 2015, Line+ 2016, Stevenson+ 2017, Wakeford+ 2017 Key Ques>on #1: What are the metallici'es of planetary atmospheres? 0.1 Line et al. (2016) Kreidberg et al. (2015) 0.01 HD 209458b WASP-43b 0.001 HD 189733b Stevenson et al. (2016) env Z 0.0001 WASP-12b 1e-05 1e-06 nominal model opac = 400 Mor opac = S+F 1e-07 300 350 400 450 500 550 600 650 700 Mplanet [M⊕] Figure from Julia Venturini based on Venturini+ 2016 Key Ques>on #2: What are the carbon-to- oxygen ra'os (C/O) in planetary atmospheres? H2O CO, CO2, CH4, C2H2, HCN, etc.? Key Ques>on #2: What are the carbon-to- oxygen ra'os (C/O) in planetary atmospheres? Note this depends strongly on temperature, pressure, and Madhusudhan 2012 metallicity. Key Ques>on #2: What are the carbon-to- oxygen ra'os (C/O) in planetary atmospheres? Jupiter from the Galileo probe Owen+ 1999 Key Ques>on #2: What are the carbon-to- oxygen ra'os (C/O) in planetary atmospheres? Öberg+ 2011 See also Madhusudhan+ 2014 Precise Water Abundance for WASP-43b dayside'emission'spectrum' transmission) emission) combined) H2O) combined)result)gives)(1σ):) transmission'spectrum' O/H)=)0.4)–)3.5)x)solar!) (assuming)solar)abundance)rADos)) Kreidberg+ 2014b Water detec'on for WASP-12b model fit by Mike Line transmission spectrum 7σ detec>on of water absorp>on First use of the G102 grism for exoplanets Kreidberg+ 2015 Key Ques>on #2: What are the carbon-to- oxygen ra'os (C/O) in planetary atmospheres? WASP-12b Results disfavor high C/O at 2σ confidence Kreidberg+ 2015 (assuming solar metallicity, chemical equilibrium, & 1D) Key Ques>on #2: What are the carbon-to- oxygen ra'os (C/O) in planetary atmospheres? WASP-12b Results disfavor high C/O at >3σ confidence Kreidberg+ 2015 (s>ll assuming chemical equilibrium & 1D) See also Benneke arXiv:1504.07655 Combining high- and low-resolu'on spectroscopy VLT CRIRES (Schwarz et al. 2016) HD 209458b Brogi+ 2017 Combining high- and low-resolu'on spectroscopy HST + Spitzer HST + Spitzer + VLT HD 209458b Brogi+ 2017 Combining high- and low-resolu'on spectroscopy HD 209458b Results in a nutshell: C/O < 1 at more than 3σ confidence C/O likely super-stellar Brogi+ 2017 Key Ques>on #3: How do planetary atmospheres transport heat? Komacek & Showman 2016 --all measurements from Spitzer-- The Global Thermal Structure of WASP-43b H2O Stevenson+ 2014b Key Ques>on #3: How do planetary atmospheres transport heat? Komacek & Showman 2016 --all measurements from Spitzer-- Key Ques>on #3: How do planetary atmospheres transport heat? Komacek & Showman 2016 with HST --all measurements from Spitzer-- dayside'emission'spectrum'Key Ques>on #3: How do planetary atmospheres transport heat? WASP%43b) dayside'emission'spectrum' fric2onal#drag:# τ#=#0#s# τ#=#1#x#105#s# τ#=#3#x#105#s# # 1x#/#5x#solar#metallicity# band1integrated'phase'curve' Kataria+ 2015 New HST/WFC3 Phase Curves WASP-103b Similar gravity and rota>on rate as WASP-43b, but much hooer (3000 vs 1700 K) Project led by Laura Kreidberg (Harvard CfA) WASP-18b Similar T as WASP-103b, but much higher gravity (10 vs 1.5 Mjup) Analysis led by Jacob Arcangeli (U. Amsterdam) Key Ques>on #3: How do planetary atmospheres transport heat? Komacek & Showman 2016 with HST --all measurements from Spitzer-- Key Ques>on #3: How do planetary atmospheres transport heat? Komacek & Showman 2016 WASP-43b WASP-18b WASP-103b Fundamental Ques'ons for Exoplanet Atmospheres What are they like? Where did they come from? Compara>ve planetology is the next step A bright future for compara've exoplanetology! HST & Spitzer: now JWST: 2018+ FINESSE: 2020s The poten>al of JWST for transit spectroscopy 5 μm MIRI The poten>al of JWST for transit spectroscopy Greene+ 2016 Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars **Proposal for the NASA MIDEX AO Dec 15, 2016** Objec've FINESSE will test theories of planetary origins and climate, transform compara>ve planetology, and open up exoplanet discovery space by performing a comprehensive, sta>s>cal, and uniform survey of exoplanet atmospheres. Strategy • Transmission spectroscopy of 500 planets • Phase-resolved emission spectroscopy of 100 planets • Focus on synergis>c science with JWST Origins | Climate | Discovery Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars **Proposal for the NASA MIDEX AO Dec 15, 2016** People • PI: Mark Swain • Mission Development & Opera>ons: Robert Green, Edward Wright, Gautam Vasisht • Science Team: Jacob Bean, Nicholas Cowan, Jonathan Fortney, Caitlin Griffith, Tiffany Kataria, Eliza Kempton, Laura Kreidberg, David Latham, Michael Line, Suvrath Mahadevan, Jorge Melendez, Julianne Moses, Gael Roudier, Evgenya Shkolnik, Adam Showman, Kevin Stevenson, Yuk Yung, Robert Zellem Origins | Climate | Discovery Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars Origins | Climate | Discovery Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars Solar Composition 1800K Opacities TiO+VO H2O CO Na+K H2S CO2 H2-H2/He CIA +H2 Ray. Scat. 50x Solar Composition 700K Opacities CH4 CO H2O CO2 H2-H2/He CIA +H2 Ray. Scat. H2S NH3 Origins | Climate | Discovery Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars Origins | Climate | Discovery Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars Origins | Climate | Discovery Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars Origins | Climate | Discovery Fast Infrared Exoplanet FINESSE Spectroscopy Survey Explorer Exploring the Diversity of New Worlds Around Other Stars Origins | Climate | Discovery Fundamental Ques'ons for Exoplanet Atmospheres What are they like? Where did they come from? Are any of them habitable? Towards Other Earths with Transit Spectroscopy REAL DATA! 2014 Kreidberg+ (2014a) GJ 1214b precision = 30 ppm Rp = 2.7 RE T = 580 K SIMULATED DATA 2019 Earth 2.0 precision = 10 ppm Rp = 1.0 RE T = 300 K N2-rich, trace H2O atmosphere.
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